Building the Hertzsprung
... tenth as massive as our sun? A: 1 billion years = 109 years B: 10 billion years = 1010 years C: 100 billion years = 1011 years D: 1 trillion years = 1012 years ...
... tenth as massive as our sun? A: 1 billion years = 109 years B: 10 billion years = 1010 years C: 100 billion years = 1011 years D: 1 trillion years = 1012 years ...
File - Science with Mrs. Schmidt
... b. some of the colors and some black lines. c. all the colors. d. all the colors and some black lines. _____ 11. What instrument breaks a star’s light into a spectrum? a. a continuous spectrum b. a telescope c. a spectrometer d. a spectrograph _____ 12. What can scientists tell about a star from its ...
... b. some of the colors and some black lines. c. all the colors. d. all the colors and some black lines. _____ 11. What instrument breaks a star’s light into a spectrum? a. a continuous spectrum b. a telescope c. a spectrometer d. a spectrograph _____ 12. What can scientists tell about a star from its ...
Birth, Lives, and Death of Stars
... the quick flashes if the bright spot was lined up with the Earth. Normal stars and white dwarfs cannot rotate fast enough because they do not have enough gravity to keep themselves together; they would spin themselves apart. Neutron stars are compact enough and strong enough to rotate that fast. The ...
... the quick flashes if the bright spot was lined up with the Earth. Normal stars and white dwarfs cannot rotate fast enough because they do not have enough gravity to keep themselves together; they would spin themselves apart. Neutron stars are compact enough and strong enough to rotate that fast. The ...
Announcements
... is occurring & whether people are responsible. – For each site, evaluate the science - Is it good or poor? ...
... is occurring & whether people are responsible. – For each site, evaluate the science - Is it good or poor? ...
The Interior Structure of Neutron Stars
... Bang! When stars, with initial masses in the range 11±1 -> ~25 M will, once they have evolved of the main sequence and burnt all their nuclear fuel (up to 56Fe), will end their main lives in a Type II Supernova and leave a neutron star (NS) remnant. Properties: From observations of binary pulsar sy ...
... Bang! When stars, with initial masses in the range 11±1 -> ~25 M will, once they have evolved of the main sequence and burnt all their nuclear fuel (up to 56Fe), will end their main lives in a Type II Supernova and leave a neutron star (NS) remnant. Properties: From observations of binary pulsar sy ...
123mt13-2a
... Two hydrogen atoms combine to form a molecule (red herring) Two hydrogen atoms collide – 3 points for this because this can happen but it does not “occur whenever” A hydrogen atom captures and electron (unphysical process) A hydrogen atom absorbs a red photon (red photons have insufficient energy to ...
... Two hydrogen atoms combine to form a molecule (red herring) Two hydrogen atoms collide – 3 points for this because this can happen but it does not “occur whenever” A hydrogen atom captures and electron (unphysical process) A hydrogen atom absorbs a red photon (red photons have insufficient energy to ...
Extension worksheet – Topic 6 - Cambridge Resources for the IB
... The luminosity of a star is accurately known but measurement of its apparent brightness is made difficult by the presence of dust in the interstellar medium. Suggest the effect this has on the measured distance to the star. ...
... The luminosity of a star is accurately known but measurement of its apparent brightness is made difficult by the presence of dust in the interstellar medium. Suggest the effect this has on the measured distance to the star. ...
My Presentation
... which one group of stars is seen. Astronomers, or scientists who study the stars, have divided the sky into 88 areas, or constellations. We often use Latin names for constellations. Latin was the language of the ancient Romans. Long ago, the people of early civilizations studied the night sky. They ...
... which one group of stars is seen. Astronomers, or scientists who study the stars, have divided the sky into 88 areas, or constellations. We often use Latin names for constellations. Latin was the language of the ancient Romans. Long ago, the people of early civilizations studied the night sky. They ...
Stars
... characters from mythology. The formations appear at different times of the year. Each season earth can view a different sets of constellations. Also the earth views a different set of constellations on the northern and southern hemispheres. Like in August they have different sets of constellations t ...
... characters from mythology. The formations appear at different times of the year. Each season earth can view a different sets of constellations. Also the earth views a different set of constellations on the northern and southern hemispheres. Like in August they have different sets of constellations t ...
UNIT VIII/B: THE EARTH IN SPACE – STARS AND GALAXIES
... i. Most of the points of light in the night sky are stars in the Milky Way 3. Understand why light years are used to measure distances in space. a. A light-year is a unit of distance (NOT TIME!!!). It is the distance that light can travel in one year. b. Light moves at a velocity of about 300,000 km ...
... i. Most of the points of light in the night sky are stars in the Milky Way 3. Understand why light years are used to measure distances in space. a. A light-year is a unit of distance (NOT TIME!!!). It is the distance that light can travel in one year. b. Light moves at a velocity of about 300,000 km ...
Kinds of Stars
... Stable State – Stars whose diameter and radiation stay the same for millions of years. Our sun is in a stable state. When fusion doesn’t balance gravity’s force, core contracts(gets hotter) and outer layers expand. Star is bigger, brighter, more surface area. ...
... Stable State – Stars whose diameter and radiation stay the same for millions of years. Our sun is in a stable state. When fusion doesn’t balance gravity’s force, core contracts(gets hotter) and outer layers expand. Star is bigger, brighter, more surface area. ...
SR Stellar Properties
... Directions: Read pages 127-129 in Prentice Hall Science Explorer, Astronomy. 1. Stars are made mostly of ________________________ and the energy that makes them shine is produced through _____________________ __________________. 2. List the four characteristics used to classify stars: a. c. b. d. 3. ...
... Directions: Read pages 127-129 in Prentice Hall Science Explorer, Astronomy. 1. Stars are made mostly of ________________________ and the energy that makes them shine is produced through _____________________ __________________. 2. List the four characteristics used to classify stars: a. c. b. d. 3. ...
supplemental materials.
... with only four basic principles we can create physical models that largely describe the energy generation, energy transport, density, and gravity of essentially any star as well as predict surface temperature and luminosity. The simplest of these principles is that the mass interior to any radius is ...
... with only four basic principles we can create physical models that largely describe the energy generation, energy transport, density, and gravity of essentially any star as well as predict surface temperature and luminosity. The simplest of these principles is that the mass interior to any radius is ...
d = 1 / p
... If we know the distances from parallax, we can remove the effect of distance and calculate the intrinsic brightness, or luminosity – the total energy the star emits per second. Imagine building a gigantic shell centered around the star, giving that shell a radius d equal to the distance between the ...
... If we know the distances from parallax, we can remove the effect of distance and calculate the intrinsic brightness, or luminosity – the total energy the star emits per second. Imagine building a gigantic shell centered around the star, giving that shell a radius d equal to the distance between the ...
Problem 4: magnitude of the star?
... index B-V=0 are all characteristics of stars with spectral type A. A0 B. B0 C. F0 D. G0 E. K0 __C___13. A star forms on the main sequence with twice the mass of our sun. It’s lifetime on the main sequence, relative to that for a solar mass star, is A. The same B. Half as long C. 1/4 as long D. 1/9 a ...
... index B-V=0 are all characteristics of stars with spectral type A. A0 B. B0 C. F0 D. G0 E. K0 __C___13. A star forms on the main sequence with twice the mass of our sun. It’s lifetime on the main sequence, relative to that for a solar mass star, is A. The same B. Half as long C. 1/4 as long D. 1/9 a ...
d = 1 / p
... If we know the distances from parallax, we can remove the effect of distance and calculate the intrinsic brightness, or luminosity – the total energy the star emits per second. Imagine building a gigantic shell centered around the star, giving that shell a radius d equal to the distance between the ...
... If we know the distances from parallax, we can remove the effect of distance and calculate the intrinsic brightness, or luminosity – the total energy the star emits per second. Imagine building a gigantic shell centered around the star, giving that shell a radius d equal to the distance between the ...
HR Diagram
... Directions: Read pages 127-129 in Prentice Hall Science Explorer, Astronomy. 1. Stars are made mostly of ________________________ and the energy that makes them shine is produced through _____________________ __________________. 2. List the four characteristics used to classify stars: a. c. b. d. 3. ...
... Directions: Read pages 127-129 in Prentice Hall Science Explorer, Astronomy. 1. Stars are made mostly of ________________________ and the energy that makes them shine is produced through _____________________ __________________. 2. List the four characteristics used to classify stars: a. c. b. d. 3. ...
1 Ay 124 Winter 2016 – HOMEWORK #3
... Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about the nucleus at 150 km s−1 . The total luminosity from within 1 arc ...
... Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about the nucleus at 150 km s−1 . The total luminosity from within 1 arc ...
Stars - Mrs. Tosh`s class
... Gravity pulls huge nebulas of hydrogen gas and dust into a single spinning cloud. As the particles crash into each other, the matter heats up….about ...
... Gravity pulls huge nebulas of hydrogen gas and dust into a single spinning cloud. As the particles crash into each other, the matter heats up….about ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.